Continuing Observations

Once you have completed a pair of main and offset beam observations, the pipeline forms a group file, into which it subtracts the main and offset images. This image is then displayed in a seperate GAIA window, the spectrum extracted from both rows in it is displayed in the top half of a second KAPPA window and the y-profile is displayed on the lower left of the first KAPPA window and mentioned above. Examples:

If this object has been flagged as a standard star (in the OT), then the pipeline will consult the BS catalogue or SIMBAD to determine the spectral type (and hence temperature) and V magnitude of the star (which are displayed in the extracted spectrum title). It will use these to create a black body model of the star (nb. no interpolation over stellar features currently takes place), which will be used to flux calibrate subsequent data.

As soon as you have observed a non standard star tagret in the main and offset beam positions, a group file will be created and displayed and spectra will be extracted and displayed as before. An additional KAPPA window is created to show you the extracted spectrum (_sp) and flux calibrated (fc) spectra. These are obviously all updated as more data is observed and signal to noise ratio is accumulated. Examples follow:

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